Coalescing binary systems of compact objects: Dynamics of angular momenta

Details Coalescing binary systems of compact objects: Dynamics of angular momenta Coalescing binary systems of compact objects: Dynamics of angular momenta

1997-09-03

arxiv.org/abs/gr-qc/9709007v2

The Astrophysical Journal, 507:287-299, 1998 November 1

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

22 pages, AASTeX and 13 figures in PostScript

Scientific paper

10.1086/306295

The end state of a coalescing binary of compact objects depends strongly on the final total mass M and angular momentum J. Since gravitational radiation emission causes a slow evolution of the binary system through quasi-circular orbits down to the innermost stable one, in this paper we examine the corresponding behavior of the ratio J/M^2 which must be less than 1(G/c) or about 0.7(G/c) for the formation of a black hole or a neutron star respectively. The results show cases for which, at the end of the inspiral phase, the conditions for black hole or neutron star formation are not satisfied. The inclusion of spin effects leads us to a study of precession equations valid also for the calculation of gravitational waveforms.

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